Proceedings of the IMC, Mistelbach, 015 197 First results of Bosnia-Herzegovina Meteor Network (BHMN) Nedim Mujić 1 and Muhamed Muminović 1 Astronomical Society Orion Sarajevo nedim_mujic@bih.net.ba Astronomical Society Orion Sarajevo and Federal Hydrometeorological Institute Sarajevo, Bosnia and Herzegovina Inspired by similar networks in the region, a video meteor network began since the spring of 013 in Bosnia and Herzegovina which currently includes eight stations. Further expansion of the network is under preparation by setting up another stations. The Network is managed by the Astronomical Society Orion Sarajevo together with the Federal Hydrometeorological Institute in Sarajevo whose meteorological stations were used for the installation of the cameras. By mid-june 015 the cameras of the BH meteor network had recorded over 0000 meteors and we had calculated more than 4000 orbits. In this paper we present the results of the first two years of operation of our meteor network. 1 Introduction The Bosnia-Herzegovina meteor network (BHMN) has been created and developed in the previous three years as a result of the work of members of the Astronomical Society Orion Sarajevo and their cooperation with the Federal Hydrometeorological Institute in Bosnia and Herzegovina. In the first phase (August 01 May 013) we tested many CCTV cameras, housings, locations and software. In May 013., we started to set up the permanent stations in BiH and neighboring countries. In this paper we present the first results of the BiH meteor network. One is at a private house in Croatia. Basic information about all the locations of stations, orientation, field of view and precision of the cameras are given in Table 4. A map of the sky coverage of the BiH stations at an altitude of 100 km is shown in Figure. Stations and equipment Many of the CCTV cameras in use today for video surveillance in low light conditions have sufficient sensitivity to detect stars up to an apparent magnitude of +4, using a high-quality lens with a field of view in the order of 80x60 degrees. Astronomers recognized these opportunities and many models of these cameras are being used to monitor star occultations by asteroids and also for capturing meteors. After a certain period of testing various models, we acquired 7 cameras from the manufacturer idea Classic from Croatia (model DVC- CAM SM34LX-Ex) and 3 cameras from the manufacturer KT & C from Korea, (model KPC-350BH). Both types of cameras use a highly sensitive Sony Super HAD CCD chip. For all of these cameras we purchased lenses from the Japanese manufacturer Tokina, model TVR0398DCIR. Specifications of the chips and camera lenses are given in Table 1. and Table. below. Each station consists of a computer, UPS and a camera placed in a housing with heating in front of the window. In cooperation with the Federal Hydrometeorological Institute of the Federation of BiH we have set up eight permanent stations so far, mainly on buildings of existing hydrometeorological stations in various cities across BiH. Figure 1 Two types of cameras and the Tokina lens.
198 Proceedings of the IMC, Mistelbach, 015 Table 1 Specifications of the chips of the cameras. model format system chip DVC-CAM- SM34LX-Ex 1/3" PAL 5 fps KPC-350BH 1/3" NTSC 9.97 fps Table Specifications of the camera lenses. model Focal length F number 0.98 Iris TVR0398DCIR 3-8. mm manual automatic ICX55AL ICX54AL rectilinear. The quality of the orbits obtained, i.e. the uncertainty of the orbital elements and atmospheric path, depend significantly on the geometry of the specific case and the duration of the meteor. The best orbits are obtained in the case that the angle between the geometric planes of the two stations is near to 90 and the velocity of the meteor can be better determined if the duration is long. Because of this, UFOOrbit classifies orbits according to certain quality criteria. The best orbits are the so-called Q3 orbits for which it is required that the angle between two planes is at least 15 and the duration is at least 0.3 seconds. In addition, the angular length of the meteor trail at both stations needs to be at least 3, they should have at least a 50% of overlap and the difference in speeds calculated from each stations should not exceed 10%. There are also some other requirements concerning the height at which the meteor appeared, its geocentric velocity and the uncertainty in the determination of the radiant. 4 Shower statistics and special cases Figure The map of the sky coverage of the BiH stations at an altitude of 100 km. 3 Acquisition and processing All cameras are monochromatic and have an analog output, hence for digitization and recording we need a TV card with video input or a special video grabber. We have various models PCI TV cards in our computers, most of them from the manufacturers Hauppauge and EasyCap USB video grabbers. The acquisition of meteor data captured by a digitized video is done with the software package UFO produced by the Japanese meteor network SonotaCo 1. This package consists of three programs: UFOCapture for the recording of meteors, UFOAnalyzer for the calibration of the cameras fields of view and the measurements of the meteor coordinates in each frame of the video and UFOOrbit to compute the atmospheric trajectory and orbit of simultaneously recorded meteors. To search for a simultaneous meteor in a video among various cameras it is essential that the system clocks of the computers at each station is synchronized. This is done with the help of the Dimension 4 software which adjusts the system time of computers via the Internet synchronized every minute with time servers. The software UFOOrbit uses the so-called Method of planes (Ceplecha, 1987) to calculate the atmospheric trajectory and orbit in which, due to their very short duration, the meteor trajectories can be considered During the period of our existence, up to August 015, the cameras of the Bosnia and Herzegovina Meteor Network have recorded a total of 6978 meteors, of which 4670 have been recorded simultaneously by two or more cameras and have calculated orbits. The recorded meteors are from all major showers and their data are given in Table 3. From these calculated orbits, 694 are of highest quality (Q3) according to the parameters of the software UFOOrbit. The projections of their atmospheric trajectories and orbits are given in Figure 3and 4. A few fireballs have been recorded bright meteors accompanied by explosions, some of which had an absolute magnitude brighter than -5. Until now, the brightest fireball was captured on 1 November 013 at 3 h 36 m 59 s UTC, recorded by 3 stations of the BH network, stations of the Croatian Meteor Network and one station of the Italian meteor network. It lasted longer than 3 seconds and started at an altitude of about 90 km and ended at about 34 km above the city Zenica. According to the analysis which is still in progress, the absolute magnitude was between -8 and -9 and the initial mass of the object may have been around 10 kilograms. Table 3 Numbers of recorded meteors for some major showers. meteor shower number of meteors number of orbits number of Q3 orbits Orionids 01. 86 33 Perseids 013. 663 84 7 Orionids 013. 333 47 3 Geminids 013. 1081 0 5 Perseids 014. 1988 410 56 Orionids 014. 501 66 Geminids 014. 1381 88 78 Perseids 015. 1711 375 77 1 http://sonotaco.com/e_index.html
Proceedings of the IMC, Mistelbach, 015 199 Table 4 Basic information about all the locations of stations, orientation, field of view and precision of the cameras. location lat E long alt (m) resolution FOV azimuth elevation Pelješac 43.07 17.0318 10.0 704x58 80x60 15.07 47.16 7.0 Bihać 44.8078 15.8667 301.0 704x58 80x60 160.37 37.66 7.0 Gradačac 44.8700 18.4500 30.5 704x58 80x60 17.15 31.0 7.0 Mostar 43.3483 17.7933 97.0 704x58 70x5 78.81 51.9 6.0 Sarajevo - Zavod 43.8676 18.48 631.0 70x480 90x68 309.57 36.71 7.5 Sarajevo - Mejtaš 43.860 18.407 578.0 704x58 70x5 137.69 41.98 6.0 Bjelašnica I 43.7038 18.571 054.0 70x480 66x44 313.55 53.60 6.0 Bjelašnica II 43.7038 18.571 054.0 70x480 66x44 84.70 44.55 6.0 '/ pixel Figure 3 Projection of the trajectories of 694 double station meteors with the highest accuracy Q3. Figure 4 Radiants of all recorded meteors.
00 Proceedings of the IMC, Mistelbach, 015 Figure 5 A bright fireball captured on 1 November 013. from the Sarajevo, Pelješac and Gradačac stations. Another bright fireball was captured on September 13 th 014 at 00 h 54 m 41 s UTC by 3 stations of the BH network. It lasted longer than 6 seconds (the longest duration up to now) and started at an altitude of about 85 km over the city Travnik and ended at about 44 km above the city Gradačac. During its flight, it showed at least 5 explosions and there is a possibility that some of the fragments survived the atmospheric flight and eventually fell in the Posavina region near the border between Bosnia and Croatia. 5 Analysis of the Geminids 013 and the Perseids 014 In the study of the small bodies of the Solar system, in particular, meteor showers, the most commonly used criterion of mutual association of orbits of small bodies and their relation to the same shower or their associations with some parent body is called the Southworth- Hawkings criteria (Southworth and Hawkins, 1963). This criteria uses the orbital elements of the body and defines the distance between two orbits as: = (e B e A ) + (q B q A ) + [sin (i B i A ) ] + sin i A sin i B [sin (Ω B Ω A ) ] + [ (e B + e A ) sin (Ω B + ω B ) (Ω A + ω A ) ] Some authors have taken different value, below which two orbits are considered to belong to the same meteor showers or can be associated with a shower or with a known parent body. For the Geminids, which are a shower with well-defined orbits and a very sharp peak of activity, the value is one of the smallest. To investigate the quality of the data that we get, thanks to very favorable weather conditions that we had during the peak of the Geminids in December 013., we decided to compare our orbits with the orbits of the Japanese meteor network SonotaCo and with the orbit of the assumed parent body of the Geminids asteroid 300 Phaeton. Table 5 shows the orbital elements for 6 Geminids recorded during the night of their maximum December 13 14 013. Only the highest quality meteors were selected for this analysis (Q3 criterion in the program UFOOrbit). The Same procedure was applied to the 014 Perseids, for which we present 0 Q3 orbits together. We compare these with the mean orbit by SonotaCo and the orbit of the parent comet 109P/Swift-Tuttle (Table 6). 6 Conclusion The activities carried out so far by the Bosnia and Herzegovina meteor network showed the extreme usability of cheap video surveillance equipment for the recording of meteors which makes serious research possible in this field. The results we get (and which we will get in the future) with this equipment and methods will enable various statistical studies of meteor showers. In addition, as a patrol network that captures every clear night, our meteor network will sooner or later register fireballs that will survive their atmospheric flight and drop meteorites. After the analysis of such event it will be possible to calculate the site of fall. We have plans to expand our meteor network by setting up new stations that will allow to improve the quality of the results.
Proceedings of the IMC, Mistelbach, 015 01 Table 5 Orbital elements for 6 Geminids recorded during the night of their maximum December 13 14, 013. n Sol a q e i ω Ω α δ V g SonotaCo Phaeton 1 61.737 1.18 0.145 0.881 1.36 35.19 61.74 113.73 31.8 3.99 0.030 0.030 61.766 1.199 0.151 0.874.5 34.67 61.77 113.94 3.50 3.66 0.017 0.033 3 61.818 1.79 0.139 0.891 4.71 35.31 61.8 114.35 3.68 34.06 0.043 0.049 4 61.81 1.94 0.151 0.884.79 33.64 61.8 113.14 3.6 33.49 0.005 0.041 5 61.85 1.84 0.147 0.886 1.39 34.7 61.83 113.06 31.86 33.45 0.04 0.035 6 61.859 1.334 0.143 0.893 1.71 34.9 61.86 11.9 31.75 34.00 0.01 0.031 7 61.877 1.301 0.154 0.88.50 33.16 61.88 11.91 3.67 33.38 0.01 0.046 8 61.879 1.3 0.146 0.890 3.8 34.06 61.88 113.33 3.49 33.96 0.013 0.038 9 61.884 1.60 0.147 0.883 1.93 34.43 61.88 113.48 3.11 33.9 0.016 0.030 10 61.891 1.4 0.139 0.90 4.9 34.19 61.89 113.16 3.40 34.99 0.035 0.049 11 61.893 1.35 0.149 0.880 1.81 34.51 61.89 113.65 3.17 33.01 0.019 0.031 1 61.907 1.95 0.146 0.888 3.37 34.31 61.91 113.63 3.54 33.77 0.015 0.036 13 61.917 1.9 0.146 0.881 1.0 34.91 61.9 113.66 31.7 33.00 0.034 0.033 14 61.935 1.31 0.154 0.875.18 33.89 61.94 113.59 3.59 3.80 0.014 0.039 15 61.941 1.366 0.146 0.893 3.51 33.61 61.94 113.06 3.56 34.6 0.017 0.043 16 61.947 1.91 0.145 0.887 1.86 34.37 61.95 113.3 31.95 33.61 0.018 0.09 17 61.950 1.364 0.146 0.893.71 33.69 61.95 11.90 3.4 34.19 0.010 0.037 18 61.978 1.331 0.140 0.895.7 34.76 61.98 113.50 31.93 34. 0.01 0.06 19 61.989 1.376 0.143 0.896 3.06 34.0 61.99 113.10 3.18 34.44 0.016 0.035 0 61.99 1.77 0.146 0.886.65 34.48 61.99 113.71 3.7 33.57 0.01 0.08 1 6.01 1.30 0.148 0.888.7 33.80 6.01 113.5 3.37 33.80 0.005 0.035 6.014 1.6 0.157 0.87.4 33.56 6.01 113.66 3.85 3.65 0.016 0.043 3 6.018 1.79 0.149 0.883.10 34.01 6.0 113.41 3.4 33.38 0.01 0.03 4 6.03 1.43 0.146 0.897 3.53 33.14 6.0 11.73 3.5 34.61 0.0 0.048 5 6.09 1.305 0.147 0.887 3.16 34.04 6.03 113.56 3.51 33.77 0.011 0.035 6 6.167 1.9 0.147 0.881.50 34.81 6.17 114.9 3.9 33.1 0.00 0.05 mean 1.96 0.147 0.887.60 34.0 61.93 113.4 3.30 33.63 0.018 0.036 std.dev. 0.061 0.004 0.007 0.88 0.56 0.09 0.41 0.3 0.61 0.009 0.007 Table 6 0 Q3 quality orbits for the 014 Perseids compared to the mean orbit by SonotaCo and the orbit of the parent comet 109P/Swift-Tuttle. n Sol a q e i ω Ω α δ V g SonotaCo Swift- Tuttle 1 137.93 11.47 0.955 0.917 113.61 151.60 137.9 44.6 56.97 58.96 0.037 0.08 138.08 15.884 0.964 0.939 113.00 154.0 138.03 43.0 57.39 59.03 0.049 0.043 3 139.000 8.38 0.956 0.886 111.53 151.49 139.00 45.15 58.34 58.00 0.056 0.093 4 139.008 14.85 0.963 0.935 115.77 153.68 139.01 45.01 56.01 59.86 0.069 0.060 5 139.008 0.861 0.964 0.954 113.41 154.6 139.01 44.39 57.49 59.31 0.064 0.0 6 139.050 0.39 0.960 0.953 114.47 153.05 139.05 45.37 56.9 59.6 0.05 0.036 7 139.103 9.57 0.956 0.900 115.74 151.69 139.10 45.98 55.95 59.48 0.060 0.089 8 139.800 14.38 0.957 0.933 114.78 15.37 139.80 46.69 56.86 59.5 0.049 0.047 9 139.88 14.585 0.958 0.934 113.97 15.51 139.83 46.5 57.35 59.8 0.044 0.037 10 139.868 11.050 0.968 0.91 11.45 155.13 139.87 44.50 58.03 58.6 0.088 0.06 11 139.961 30.561 0.960 0.969 11.47 153.31 139.96 46.7 58.45 59.15 0.069 0.01 1 139.968 3.765 0.959 0.971 110.80 153.01 139.97 46.3 59.48 58.6 0.076 0.038 13 140.00 0.468 0.95 0.953 113.0 151.18 140.0 47.70 58.01 59.0 0.031 0.034 14 140.058 4.11 0.960 0.960 113.90 153.11 140.06 46.69 57.58 59.5 0.064 0.018 15 140.059 10.134 0.95 0.906 113.41 150.79 140.06 47.54 57.65 58.80 0.031 0.069 16 140.886 8.015 0.953 0.881 113.9 150.8 140.89 48.39 57.79 58.5 0.061 0.087 17 140.911 13.99 0.956 0.93 114.07 151.97 140.91 48.35 57.58 59.9 0.055 0.041 18 140.961.483 0.949 0.958 113.66 150.49 140.96 49.56 58.03 59.39 0.04 0.036 19 141.075 16.370 0.944 0.94 114.04 149.3 141.08 50.34 57.77 59.34 0.09 0.057 0 14.867 1.708 0.947 0.96 113.33 149.8 14.87 5.3 58.54 58.98 0.066 0.06 mean 16.649 0.957 0.933 113.55 15.18 139.87 46.71 57.61 59.13 0.055 0.051 std.dev. 6.955 0.006 0.06 1.0 1.54 1.14.7 0.83 0.44 0.016 0.04
0 Proceedings of the IMC, Mistelbach, 015 Finally the educational aspects of this work are also important. In activities of this network we include secondary school pupils or students of natural sciences who can conduct initial analysis allowing them to make a first experiences in serious scientific research. References Ceplecha Z. (1987). Geometric, dynamic, orbital and photometric data on meteoroids from photographic fireball networks. Bulletin of the Astronomical Institutes of Czechoslovakia, 38, 34. Southworth R. B. and Hawkins G. S. (1963). Statistics of meteor streams. Smithsonian Contributions to Astrophysics, 7, 61 85. Veres P. and Toth J. (010). Analysis of the SonotaCo video meteoroid orbits. WGN, Journal of the IMO, 38, 54 57. Nedim Mujić during his presentation (Photo by Axel Haas).